Dual Nature of the Solar Wind Quasi-Invariant

Details Dual Nature of the Solar Wind Quasi-Invariant Dual Nature of the Solar Wind Quasi-Invariant

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh31a0707f&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH31A-0707

Other

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2162 Solar Cycle Variations (7536), 2164 Solar Wind Plasma

Scientific paper

Since the beginning of the space age numerous attempts have been made to relate solar wind parameters such as magnetic field B, solar wind speed v, density ρ and others to sunspot numbers (SSN) (see for example, Slavin et al. [1986] and King [1979]). Recently it has been demonstrated that the solar wind quasi-invariant (B2/8π )/(ρ v2/2) followed the yearly sunspot numbers with a correlation coefficient = 0.98 (Osherovich, Fainberg and Stone, [1999]) for 28 years. Similar results for the 10 year period of Pioneer-Venus Orbiter (Fainberg, Osherovich and Stone, 2001) confirmed the global nature of QI as a new heliospheric index of solar activity. For interplanetary clouds, QI increases by at least an order of magnitude because of the magnetic field enhancement and the depletion due to expansion. Thus, short term variations of QI (days, hours) allow detection and classification of geo-effective interplanetary disturbances such as magnetic clouds. While SSN cannot help in describing and forecasting individual geo-effective events, QI is suitable for such tasks. With data from Wind, Ulysses and other spacecraft, we will illustrate the application of QI in describing the level of long (years) and short term solar activity. References: Fainberg, J, V Osherovich and R G Stone, GRL, 28(8), 1447, 2001. King, J H, JGR, 84, 5938, 1979. Osherovich, V, J Fainberg and R G Stone, GRL, 26(16), 2597, 1999. Slavin, J A, G Jungman and E J Smith, GRL, 13, 6, 513, 1986.

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